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Fast evaluation of multi-detector consistency for real-time gravitational wave searches

Hanna, Chad and Caudill, Sarah and Messick, Cody and Sachdev, Surabhi and Cannon, Kipp and Blackburn, Kent and Creighton, Jolien D. E. and Fong, Heather and Godwin, Patrick and Kapadia, Shasvath and Li, Tjonnie G. F. and Magee, Ryan and Meacher, Duncan and Mukherjee, Debnandini and Pace, Alex and Privitera, Stephen and Lo, Rico K. L. and Wade, Leslie (2019) Fast evaluation of multi-detector consistency for real-time gravitational wave searches. . (Unpublished)

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Gravitational waves searches for compact binary mergers with LIGO and Virgo are presently a two stage process. First, a gravitational wave signal is identified. Then, an exhaustive search over signal parameters is performed. The identification stage must be efficient in order to maximize the number of gravitational wave sources that are identified. Initial identification of gravitational wave signals with LIGO and Virgo happens in real-time, which requires that less than one second of computational time must be used for each second of gravitational wave data collected. In contrast, subsequent parameter estimation may require hundreds of hours of computational time to analyze the same one second of gravitational wave data. The real-time identification requirement necessitates efficient and often approximate methods for signal analysis. We describe one piece of a real-time gravitational-wave identification algorithm: an efficient method for ascertaining a signal's consistency between multiple gravitational wave detectors. This technique was used in analyses of Advanced LIGO's second observing run and Advanced Virgo's first observing run.

Item Type:Report or Paper (Discussion Paper)
Related URLs:
URLURL TypeDescription Paper
Caudill, Sarah0000-0002-8927-6673
Messick, Cody0000-0002-8230-3309
Cannon, Kipp0000-0003-4068-6572
Blackburn, Kent0000-0002-3838-2986
Li, Tjonnie G. F.0000-0003-4297-7365
Additional Information:This work was supported by the National Science Foundation through PHY-1454389, OAC-1841480, PHY-1700765, and PHY-1607585. Funding for this project was provided by the Charles E. Kaufman Foundation of The Pittsburgh Foundation. We thank the LIGO Scientific Collaboration for input on this work. Specifically, CH would like to thank Patrick Brady for several illuminating discussions. This research was supported in part by Perimeter Institute for Theoretical Physics. Research at Perimeter Institute is supported by the Government of Canada through the Department of Innovation, Science, and Economic Development, and by the Province of Ontario through the Ministry of Research and Innovation. Computations for this research were performed on the Pennsylvania State University's Institute for Cyber-Science Advanced CyberInfrastructure (ICS-ACI). We are grateful for computational resources provided by the Leonard E Parker Center for Gravitation, Cosmology and Astrophysics at the University of Wisconsin-Milwaukee and supported by National Science Foundation Grants PHY-1626190 and PHY-1700765. The authors are grateful for computational resources provided by the LIGO Laboratory and supported by National Science Foundation Grants PHY-0757058 and PHY-0823459. This paper has LIGO document number: P1800362.
Funding AgencyGrant Number
Charles E. Kaufman FoundationUNSPECIFIED
Pittsburgh FoundationUNSPECIFIED
Perimeter Institute for Theoretical PhysicsUNSPECIFIED
Department of Innovation, Science and Economic Development (Canada)UNSPECIFIED
Ontario Ministry of Research and InnovationUNSPECIFIED
Other Numbering System:
Other Numbering System NameOther Numbering System ID
LIGO DocumentP1800362
Record Number:CaltechAUTHORS:20190501-135957305
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:95142
Deposited By: George Porter
Deposited On:01 May 2019 22:06
Last Modified:03 Oct 2019 21:10

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